On the Use of Field RR Lyrae as Galactic Probes. I. The Oosterhoff Dichotomy Based on Fundamental Variables Partially based on observations collected under ESO programs 297.D-5047 (PI: G. Bono) and 083.B-0281 (PI: D. Romano).

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dc.contributor.authorFabrizio M.
dc.contributor.authorBono G.
dc.contributor.authorBraga V.F.
dc.contributor.authorMagurno D.
dc.contributor.authorMarinoni S.
dc.contributor.authorMarrese P.M.
dc.contributor.authorFerraro I.
dc.contributor.authorFiorentino G.
dc.contributor.authorGiuffrida G.
dc.contributor.authorIannicola G.
dc.date.accessioned2024-06-24T19:22:03Z
dc.date.available2024-06-24T19:22:03Z
dc.date.issued2019-09-10
dc.descriptionIndexación: Scopus.
dc.description.abstractWe collected a large data set of field RR Lyrae stars (RRLs) by using catalogs already available in the literature and Gaia DR2. We estimated the iron abundances for a subsample of 2382 fundamental RRLs (ΔS method: Ca ii K, Hβ, Hγ, and Hδ lines) for which there are publicly available medium-resolution SDSS-SEGUE spectra. We also included similar estimates available in the literature, ending up with the largest and most homogeneous spectroscopic data set ever collected for RRLs (2903). The metallicity scale was validated by using iron abundances based on high-resolution spectra for a fundamental field RRL (V Ind), for which we collected X-shooter spectra covering the entire pulsation cycle. The peak ([Fe/H] =-1.59 ± 0.01) and the standard deviation (σ = 0.43 dex) of the metallicity distribution agree quite well with similar estimates available in the literature. The current measurements disclose a well-defined metal-rich tail approaching solar iron abundance. The spectroscopic sample plotted in the Bailey diagram (period versus luminosity amplitude) shows a steady variation when moving from the metal-poor ([Fe/H] =-3.0/-2.5) to the metal-rich ([Fe/H] =-0.5/0.0) regime. The smooth transition in the peak of the period distribution as a function of the metallicity strongly indicates that the long-standing problem of the Oosterhoff dichotomy among Galactic globular clusters is the consequence of the lack of metal-intermediate clusters hosting RRLs. We also found that the luminosity amplitude, in contrast with period, does not show a solid correlation with metallicity. This suggests that period-amplitude-metallicity relations should be cautiously treated.
dc.description.urihttps://iopscience.iop.org/article/10.3847/1538-4357/ab3977/pdf
dc.identifier.citationAstrophysical Journal Volume 882, Issue 2 10 September 2019 Article number 169
dc.identifier.doi10.3847/1538-4357/ab3977
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.unab.cl/handle/ria/57945
dc.language.isoen_US
dc.publisherInstitute of Physics Publishing
dc.rights.licenseATRIBUCIÓN 4.0 INTERNACIONAL
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/deed.es
dc.subjectGalaxy: Halo-stars: Variables: Rr lyrae-techniques: Spectroscopic
dc.titleOn the Use of Field RR Lyrae as Galactic Probes. I. The Oosterhoff Dichotomy Based on Fundamental Variables Partially based on observations collected under ESO programs 297.D-5047 (PI: G. Bono) and 083.B-0281 (PI: D. Romano).
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